on dust in the early universe
DESCRIPTION
On Dust in the Early Universe. Takaya Nozawa (IPMU, University of Tokyo). Contents: 1. Observations of dust at high-z 2. Formation of dust in supernovae 3. Critical metallicity 4. EMP-stars and dust. 2010/07/29. 1. Observations of dust at high-z. - PowerPoint PPT PresentationTRANSCRIPT
![Page 1: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/1.jpg)
On Dust in the Early UniverseTakaya Nozawa
(IPMU, University of Tokyo)
2010/07/29
Contents:
1. Observations of dust at high-z
2. Formation of dust in supernovae
3. Critical metallicity
4. EMP-stars and dust
![Page 2: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/2.jpg)
1. Observations of dust at high-z
![Page 3: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/3.jpg)
・ The submm observations have confirmed the presence of dust in excess of 10^8 Msun in 30% of z > 5 quasars ➔ We see warm dust grains heated by absorbing stellar lights in the host galaxies of the quasars
Robson+04, MNRAS, 351, L29
SDSS J1148+5251 at z=6.4
1-1. Discovery of large amounts of dust at z > 5
LIR>10^13 Lsun
Wang+08, ApJ, 687, 848
180 K, β=0
40 K, β=2
![Page 4: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/4.jpg)
・ Type II SNe arising from short-lived massive stars
- ~0.1 Msun per SN (Maiolino+06, MmSAI, 77, 643)
- > 1 Msun per SN (Dwek+07, ApJ, 662, 927)
- sufficient only with SN-dust (Li+08, ApJ, 678, 41)
・ AGB stars are more dominant than SNe (50-80 %)
(Valiante+09, MNRAS, 397, 1661)
➔ ~0.01 Msun per AGB, ~0.05 Msun per SN
・ grain growth in the ISM
(Draine 2009, arXiv:0903.1658)
・ quasar outflow
(Elvis+02, ApJ, 567, L107)
1-2. What are sources of dust in z =6.4 quasar?
![Page 5: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/5.jpg)
1-3. Herschel Observations of z=6.4 quasar
Leipski+10 (arXiv:1005.5016)
*Herschel (3.5m) ・ PACS : 70, 100, 160 μm
・ SPIRE 250, 350, 500 μm
・ a broad range of dust temperature (LIR > 10^14 Lsun)
・ Another source northwest of the QSO J1148+5251 at z=6.4 is clearly visible
z=6.4 z=4.7
![Page 6: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/6.jpg)
1-4. Sources of dust in 5 < z < 6.4
Grain growth in the ISM is required for at least 3 out of 9 QSOs at z > 5
Michalowski+10 (arXiv:1006.5466)
![Page 7: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/7.jpg)
1-5. Dust production in submm galaxies at z > 4
Yoshida (2010)
Population synthesis (GRASIL) ・ average SFR : ~2500 Msun/yr ・ stellar mass : ~3.6x10^11 Msun
・ dust mass : ~6.7x10^8 Msun
・ gas-to dust ratio : ~60
Dominant dust sources ・ AGB stars for three ・ SNe (0.15-0.65 Msun) for three
Michalowski+10, ApJ, 712, 942
![Page 8: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/8.jpg)
Santini+10 (arXiv:1005.5678)using Herschel/PACS and GRASIL
・ overdense region of LBGs (9 objects) at z=5.16 Non-detection at 870 μm ➔ Mdust < 1.2 x 10^8 Msun
1-6. Dust mass in submm galaxies at 2 < z < 4
Stanway+10 (arXiv:1007.0440)
![Page 9: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/9.jpg)
Maiolino+04, Nature, 431, 533
Broad absorption line (BAL) quasars
SDSS J1048+4637 at z=6.2
1-7. Extinction curves at high-z quasars
different dust properties from those at low redshifts
![Page 10: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/10.jpg)
Stratta+07, ApJ, 661, L9
Perley+09 (arXiv:0912.2999)
GRB 050904 at z=6.3
1-8. Extinction curves from high-z GRBsGRB 071025 at z~5
additional evidence for different dust properties at high-z (z > 5) but see Zafar+10, A&A, 514, 94
![Page 11: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/11.jpg)
1-9. Extinction curves at 3.9 < z < 6.4
The mean Extinction curves for BAL quasarsdeviates from the SMC with level > 95 %
Gallerani+10(arXiv:1006.4463)
7 of 33 requires substantial dust extinction, which deviates from the SMC
![Page 12: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/12.jpg)
・ what are the main sources of a huge amount
dust grains at z > 4 ➔ SNe? AGB stars? grain growth in the ISM?
quasar outflow? mass-loss winds of massive stars?
how about PISNe? any other sources?
・ Properties of dust at high-z are likely to be
different from those at low-z ➔ Is there really no extinction in many high-z quasar
systems?
・ Are there massive dust in primeval galaxies such
as LBGs?
1-10. Concluding remarks
![Page 13: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/13.jpg)
2. Formation of dust in SNe
![Page 14: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/14.jpg)
2-1. Theory vs. Observation SNe are important sources of interstellar dust?
・ Theoretical studies - before destruction : 0.08-2 Msun in Type II-P SNe (Todini & Ferrara 2001; Nozawa et al. 2003)
- after destruction : 0.01-0.1 Msun (Bianchi & Schneider 2007)
0.08-0.8 Msun (Nozawa et al. 2007)
・ Observational works - IR observations of dust-forming SNe : < 10-2 Msun (e.g., Meikle et al. 2007, Kotak et al. 2009) - submm observations of SNRs : ~1 Msun (Dunne et al. 2003; Morgan et al. 2003)
- FIR obdervation of Cas A : 0.03-0.075 Msun (Sibthorpe et al. 2009; Barlow et al. 2010)
![Page 15: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/15.jpg)
2-2. Dust formation in primordial SNeNozawa+03, ApJ, 598, 785 ・ nucleation and grain growth theory (Kozasa & Hasegawa
1988)
・ no mixing of elements within the He-core
・ complete formation of CO and SiO, sticking probability=1
〇 Population III SNe model (Umeda & Nomoto 2002)
・ SNe II-P : MZAMS = 13, 20, 25, 30 Msun (E51=1)
・ PISNe : MZAMS = 170 Msun (E51=20), 200 Msun (E51=28)
Menv ~ 12 Msun Menv ~ 90 Msun
![Page 16: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/16.jpg)
2-3. Size distribution spectrum of dust
・ grain radii range from a few A up to 1 μm ・ average dust radius is smaller for PISNe than SNe II-
P
amount of newly formed dust grains SNe II-P : Mdust = 0.1-1 Msun, fdep = Mdust / Mmetal = 0.2-0.3 PISNe : Mdust =20-40 Msun, fdep = Mdust / Mmetal = 0.3-0.4
![Page 17: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/17.jpg)
2-4. Total mass and size of surviving dust
Total dust mass surviving the destruction in Type II-P SNRs; 0.08-0.8 Msun (nH,0 = 0.1-1 cm-3)
Nozawa+07, ApJ, 666, 955
Size distribution of surviving dust is domimated by large grains (> 0.01 μm)
![Page 18: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/18.jpg)
2-5. Flattened extinction curves at high-z
Hirashita+10, MNRAS, 404, 1437
z=0.69z=4z=0.54z=1.16
Hirashita+08, MNRAS, 384, 1725
Maiolino+04, A&A, 420, 889
z=5.8, BAL z=5.1, BAL
Shattering enhances small grainsat Z=Zsun
![Page 19: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/19.jpg)
2-6. Dust formation in Type IIb SN
○ SN IIb model (SN1993J-like model) - MH-env = 0.08 Msun
MZAMS = 18 Msun Meje = 2.94 Msun
- E51 = 1, M(56Ni) = 0.07 Msun
Nozawa+10, ApJ, 713, 356
・ SN IIb without massive H-env ➔ adust < 0.01 μm
・ SN II-P with massive H-env ➔ adust > 0.01 μm
average radius
0.01 μm
![Page 20: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/20.jpg)
2-7. Destruction of dust in Type IIb SNR
Almost all newly formed grains are destroyed in shocked gas within the SNR for CSM gas density of nH > 0.1 /cc ➔ small radius of newly formed dust ➔ early arrival of the reverse shock at the He core
nH,1 = 30, 120, 200 /cc ➔ dM/dt = 2.0, 8.0, 13x10-5 Msun/yr for vw=10 km/s
constant-density CSM stellar-wind CSM
330 yr
total mass of dust formed : 0.167 Msun
![Page 21: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/21.jpg)
observed IR SED can be well reproduced !
↑ ・ Md,warm ~ 0.008 Msun
・ Md,cool ~ 0.072 Msun
with Tdust ~ 40 K
AKARI reduced 90μm image ➔ centrally peaked cool dust component
↓ Md,cool = 0.03-0.06 Msun with Tdust = 33-41 K
Sibthorpe+09 (arXiv:0910.1094)
2-8. Comparison with observations of Cas A
![Page 22: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/22.jpg)
confirmation of a cool dust component emitting at 70-160 μm inside reverse shock
↓ Md,cool = 0.075 Msun Td ~ 35 K
Barlow+10, A&A, 518, L138
2-9. Herschel observations of Cas A
・ Md,warm ~ 0.008 Msun
・ Md,cool ~ 0.072 Msun
with Tdust ~ 40 K
![Page 23: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/23.jpg)
・ Type II SNe and PISNe Average grain radii are larger than 0.01 μm
➔ primordial SNe may be important sources of dust
・ Type IIb, Type Ib/Ic, and Type Ia SNe Average grain radii are smaller than 0.01 μm
➔ envelope-stripped SNe may not be major sources
of dust
・ Extinction curves in the early universe are
expected to be flat
・ Model of dust destruction in Type IIb SNR can
well reproduce the observed SED of Cas A
2-10. Conclusion remarks
![Page 24: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/24.jpg)
3. Critical metallicity
![Page 25: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/25.jpg)
First (Pop III) star : very massive > 10-100 Msun
➔ when low-mass population II stars can form?
・ Atomic cooling - Z ~ 10^-3.5 Zsun
(Bromm+01, MNRAS, 328, 969)
- [C/H] = -3.5, [O/H] = -3.05 (Bromm & Loeb 2003, Nature, 425, 812)
- extending to [C, O, Si, Fe/H] (Santoro & Shull 2006, ApJ, 643, 26)
- Z > 10^-3 Zsun (numerical simulation) (Smith+07, 661, L5)
- Z ~ 10^-3.5 Zsun (cooling by molecules) (Jappsen+09, ApJ, 696, 1065)
3-1. Critical metallicity
![Page 26: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/26.jpg)
3-2. Minimum stellar metallicity
Frebel+09, MNRAS, 392, L50
![Page 27: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/27.jpg)
• γ< 1 vigorous fragmentation, γ >1 fragmentation suppressed
• The Jeans mass at γ~1 (T minimum) gives the fragmentation scale.
Mfrag=MJeans@
(isothermal)
Li et al. 2003
Effective ratio of specific heat
:= dlog p/dlog
3-3. Thermal evolution of gas clouds
![Page 28: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/28.jpg)
3-4. Thermal evolution of gas clouds
Omukai+05, ApJ, 626, 627
・ Dust cooling causes a sudden temperature drop at high density where MJeans~0.1 Msun, which induces low-mass fragmentation
・ low-mass fragments are formed only in the dust- induced mode
line-
indu
ced
dust-induce
d
・ one-zone model・ dust model : Pollack+94・ dust/metal ratio : same as local ISM
![Page 29: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/29.jpg)
3-5. Dust from the first stars
Dust from SNe ➔ larger area per unit dust mass (smaller radius) ➔ more refractory composition (silicates, amorphous carbon)
Schneider+06, MNRAS, 369, 1437
Zcr ~ 10-6 Zsun
progenitor: SN II (22 Msun)progenitor: PISNe (195 Msun)
![Page 30: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/30.jpg)
3-6. Fragmentation of SN shell
Nagakura+09, MNRAS,399, 2183
![Page 31: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/31.jpg)
3-7. CMB can affect fragmentation mass Schneider+10, MNRAS, 369, 1437
![Page 32: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/32.jpg)
Tsuribe & Omukai 2005, 642, L61Tsuribe & Omukai 2008, 676, L45
・ ρ-T evolution given by one- zone model for PISN-dust
[M/H]=-5.5 (Z=3x10-6 Zsun)
Z >~10-6 Zsun
➔ long filament forms during dust-cooling phase
➔ fragmentation into low-mass (0.1-1 Msun) objects
Zcr ~ 10-6-10-5 Zsun
3-8. 3D-simulation of cloud fragmentation (1)
![Page 33: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/33.jpg)
3-9. 3D-simulation of cloud fragmentation (2) Yoshida (2010)
・ Z = 10^-5 Zsun
No fragmentation
・ Z = 10^-4 Zsun
fragmentation fragment mass ~ 0.1 Msun
![Page 34: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/34.jpg)
・ Critical metallicity (induced by dust) is likely to be Z = 10^-6 to 10^-4 Zsun
3-10. Concluding remarks
![Page 35: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/35.jpg)
4. EMP-stars and dust
![Page 36: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/36.jpg)
4-1. Peculiar abundances of EMP stars Vankatesan+06, ApJ, 640, 31
![Page 37: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/37.jpg)
4-2. Chemically peculiar stars Venn+08, ApJ, 677, 572
・ preferential removal of metals by dust formation・ dilution by the accretion of metal-poor interstellar gas
![Page 38: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/38.jpg)
4-3. Radiative transport of dust Vankatesan+06, ApJ, 640, 31
Dust formed in the first SN is transported to SN shells,
and some results of segregated grain transport can
reproduce elemental composition of EMP stars
![Page 39: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/39.jpg)
The evolution of dust heavily depends on the initial radius and chemicalcomposition
aini = 0.01 μm (dotted) ➔ completely destroyed
aini = 0.1 μm (solid) ➔ trapped in the shell
aini = 1 μm (dashed) ➔ injected into the ISM
Model : Mpr=20 Msun (E51=1),
nH,0 = 1 cm-3
4-4. Evolution of dust within SNRsNozawa+07, ApJ, 666, 955
![Page 40: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/40.jpg)
metallicity of shell
Z > Zcr = 10-6 Z☉☉
[Fe/H] = -5.62 (HE0107-5240; Collet et al. 2006)[Fe/H] = -5.96 (HE1327-2326; Frebel et al. 2008)[Fe/H] = -4.75 (HE0557-4840; Noris et al. 2007) 3-D corrected
4-5. Elemental abundance in the SNR shell (1)
![Page 41: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/41.jpg)
4-6. Elemental abundance in the SNR shell (2)
- 6 < [Fe/H] <-5 0 < [Mg, Si/Fe] <2
↓elemental composi-tion of dust piled up in the shell can re- produce abundance pattern in HMP stars
Nozawa+09 (arXiv:0812.1448)
The transport of dust segregated from metal-rich gas can be responsible for the elemental composition of Population II.5 stars formed in the dense SN shell
![Page 42: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/42.jpg)
4-7. Elemental abundance of dwarf galaxies (1)
Tolstoy+10, ARAA, 47, 371
![Page 43: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/43.jpg)
4-8. Elemental abundance of dwarf galaxies (2)
Tolstoy+10
![Page 44: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/44.jpg)
4-9. Confirmation of IGM dust in galaxy halo
Menard (2010)
How dust grains are transported to the IGM?
![Page 45: On Dust in the Early Universe](https://reader035.vdocuments.mx/reader035/viewer/2022062409/56814c52550346895db96520/html5/thumbnails/45.jpg)
4-10. Concluding remarks